Flybys in protoplanetary discs: I. Gas and dust dynamics
Flybys in protoplanetary discs: I. Gas and dust dynamics
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DOI：
10.1093/mnras/sty3325
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发表时间：
2018-12
影响因子：
4.8
通讯作者：
N. Cuello;G. Dipierro;D. Mentiplay;Daniel J. Price;C. Pinte;J. Cuadra;G. Laibe;F. Ménard;P. Poblete;M. Montesinos
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文献类型：
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作者：
N. Cuello;G. Dipierro;D. Mentiplay;Daniel J. Price;C. Pinte;J. Cuadra;G. Laibe;F. Ménard;P. Poblete;M. Montesinos
我们提出了 3D 平滑粒子流体动力学模拟，对原行星盘进行 3D 平滑粒子流体动力学模拟，该原行星盘在抛物线轨道上由恒星扰动器飞越，轨道位于相对于盘中面倾斜的平面上。我们将圆盘建模为气体和灰尘的混合物，颗粒尺寸从 1 {\mu}m 到 10 cm 不等。通过探索不同的轨道倾角、近星体距离和质量比，我们研究了飞越期间和之后的盘动力学响应。我们发现，飞越会引起气体和尘埃中螺旋结构的演变，这种结构可以在近星周后持续数千年。由于对尘埃颗粒的阻力作用，飞越引起的气体和尘埃结构有所不同。吸积率的变化在 10 年或更短的时间范围内会发生高达一个数量级的变化，从而引发类似 FU Orionis 的爆发。剩余的圆盘被截断和扭曲。尘埃盘比气体盘更紧凑，这既是因为盘截断，又是由于飞越引起的颗粒径向漂移加速。
We present 3D smoothed particle hydrodynamics simulations of protoplanetary discs undergoing a flyby by a stellar perturber on a parabolic orbit lying in a plane inclined relative to the disc mid-plane. We model the disc as a mixture of gas and dust, with grains ranging from 1 {\mu}m to 10 cm in size. Exploring different orbital inclinations, periastron distances and mass ratios, we investigate the disc dynamical response during and after the flyby. We find that flybys induce evolving spiral structure in both gas and dust which can persist for thousands of years after periastron. Gas and dust structures induced by the flyby differ because of drag-induced effects on the dust grains. Variations in the accretion rate by up to an order of magnitude occur over a time-scale of order 10 years or less, inducing FU Orionis-like outbursts. The remnant discs are truncated and warped. The dust disc is left more compact than the gas disc, both because of disc truncation and accelerated radial drift of grains induced by the flyby.